Optical performance of prototype horn-coupled TES bolometer arrays for SAFARI

Audley, M. D.; Lange, Gert de; Gao, J. R.; Khosropanah, P.; Hijmering, R. A.; Ridder, M.

doi:10.1117/12.2231088

Cited by 3 publications

(5 citation statements)

References 10 publications

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“…High-performance photon sensors for future astronomical instruments are typically cooled to 100 mK or below in a dilution cryostat 33,34 . However, the cost and complexity of these units are an obstacle to the widespread use of 100 mK sensors.…”

Section: Discussionmentioning

confidence: 99%

Photon-noise-limited cold-electron bolometer based on strong electron self-cooling for high-performance cosmology missions

et al. 2019

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Bolometers for balloon and space missions have seen extensive development because of their capacity to test primordial conditions of the Universe. The major improvements consist in lowering the operating temperature to reach higher sensitivities. Here we show that an array of 192 cold-electron bolometers (CEB) demonstrates photon-noise-limited operation at the cryostat temperature of 310 mK due to effective self-cooling of the absorber. The direct electron cooling of nanoabsorber placed between normal metal-insulator-superconductor junctions has considerably higher efficiency than indirect cooling through massive suspended platform, that requires overcoming a weak electron-phonon conductance. The electron temperature reached 120 mK without a power load, and 225 mK with a 60 pW power load with self-noise of a single bolometer below 3 Á 10 À18 W Hz À1=2 at a 0.01 pW power load. This bolometer works at electron temperature less than phonon temperature, thus being a good candidate for future space missions without the use of dilution refrigerators.

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Section: Discussionmentioning

confidence: 99%

Photon-noise-limited cold-electron bolometer based on strong electron self-cooling for high-performance cosmology missions

et al. 2019

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“…The fabrication technologies used for TES bolometers are flexible as can be made with photolithographic processes and, therefore, specialized detectors and large arrays of TES sensors (see, e.g., [154,155]) can be designed to meet the needs of specific observations. The impedance of a TES is low, so it can deliver significant power only to low-input impedance amplifiers, which rules out JFETs and MOSFETs.…”

Section: Tes Superconductive Bolometersmentioning

confidence: 99%

“…Proposed space missions using TES bolometer arrays include, e.g., SPIRIT [156]; SPICA-BLISS [157]; SPICA-SAFARI [151,154,158]; LiteBIRD [159].…”

Section: Tes Superconductive Bolometersmentioning

confidence: 99%

Terahertz radiation detectors: the state-of-the-art

Sizov¹

2018

Semicond. Sci. Technol.

116

106

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The phenomena and recent progress in the evolution of the basic classes of the THz detectors that exist today are considered. Issues associated with the development and exploitation of THz radiation detectors in human activity applications are briefly addressed. The operation conditions of the THz detectors and their upper limit performance are discussed. Because of lack of space not all the important references will be mentioned. Where reasonable, mainly publications after 2011 are addressed.

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“…The Very Long Wavelength Grating module is shown in the right panel of Figure 11 as an example of the GM design. SAFARI employs the latest generation of ultrasensitive TES to detect the incoming photons Audley et al, 2016;Suzuki et al, 2016;Goldie et al, 2012;Beyer et al, 2012). TES bolometers fabricated at SRON have already demonstrated the required NEP , as well as the required optical efficiency (Audley et al, 2016).…”

Section: The Safari Detector Grating Modulesmentioning

confidence: 99%

“…SAFARI employs the latest generation of ultra-sensitive TES to detect the incoming photons (Khosropanah et al 2016;Audley et al 2016;Suzuki et al 2016;Goldie et al 2012;Beyer et al 2012). TES bolometers fabricated at SRON (Ridder et al 2016) have already demonstrated the required NEP (Khosropanah et al 2016), as well as the required optical efficiency (Audley et al 2016). To achieve their performance, the detectors, their readout, and the first-stage amplifiers must be operated at 50-mK, which requires that both the sensors and the cold electronics be cooled and thermally isolated from the 1.8-K environment of the GM.…”

Section: The Safari Detector Grating Modulesmentioning

confidence: 99%

SPICA—A Large Cryogenic Infrared Space Telescope: Unveiling the Obscured Universe

Roelfsema

Shibai

Armus

et al. 2018

Publ. Astron. Soc. Aust.

104

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Measurements in the infrared wavelength domain allow us to assess directly the physical state and energy balance of cool matter in space, thus enabling the detailed study of the various processes that govern the formation and early evolution of stars and planetary systems in the Milky Way and of galaxies over cosmic time. Previous infrared missions, from IRAS to Herschel, have revealed a great deal about the obscured Universe, but sensitivity has been limited because up to now it has not been possible to fly a telescope that is both large and cold. Such a facility is essential to address key astrophysical questions, especially concerning galaxy evolution and the development of planetary systems.SPICA is a mission concept aimed at taking the next step in mid-and far-infrared observational capability by combining a large and cold telescope with instruments employing state-of-the-art ultrasensitive detectors. The mission concept foresees a 2.5-meter diameter telescope cooled to below 8 K. Rather than using liquid cryogen, a combination of passive cooling and mechanical coolers will be used to cool both the telescope and the instruments. With cooling not dependent on a limited cryogen supply, the mission lifetime can extend significantly beyond the required three years. The combination of low telescope background and instruments with state-of-the-art detectors means that SPICA can provide a huge advance on the capabilities of previous missions.The SPICA instrument complement offers spectral resolving power ranging from R ∼50 through 11000 in the 17-230 µm domain as well as R ∼28.000 spectroscopy between 12 and 18 µm. Additionally SPICA will be capable of efficient 30-37 µm broad band mapping, and small field spectroscopic and polarimetric imaging in the 100-350 µm range. SPICA will enable far infrared spectroscopy with an unprecedented sensitivity of ∼ 5 × 10 −20 W/m 2 (5σ/1hr) -at least two orders of magnitude improvement over what has been attained to date. With this exceptional leap in performance, new domains in infrared astronomy will become accessible, allowing us, for example, to unravel definitively galaxy evolution and metal production over cosmic time, to study dust formation and evolution from very early epochs onwards, and to trace the formation history of planetary systems.

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Optical performance of prototype horn-coupled TES bolometer arrays for SAFARI

Cited by 3 publications

References 10 publications

Photon-noise-limited cold-electron bolometer based on strong electron self-cooling for high-performance cosmology missions

Photon-noise-limited cold-electron bolometer based on strong electron self-cooling for high-performance cosmology missions

Terahertz radiation detectors: the state-of-the-art

SPICA—A Large Cryogenic Infrared Space Telescope: Unveiling the Obscured Universe

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